Difference between revisions of "April 18, 2004"
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| − | + | <td colspan="2"><div align="center"> | |
| − | + | [[File:LPOD-2004-04-18.jpeg|LPOD-2004-04-18.jpeg]]</div> | |
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| − | + | <td><div align="center" span class="main_sm">Image Credit: [mailto:kcpaulhk@yahoo.com.hk K.C. Pau]</div></td> | |
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<table class="story" border="0" bgcolor="#FFFFFF" width="90%" cellpadding="10" align="center"><tr><td> | <table class="story" border="0" bgcolor="#FFFFFF" width="90%" cellpadding="10" align="center"><tr><td> | ||
| − | + | <p class="story" align="center"><b>Langrenus </b></p> | |
| − | + | <p class="story" align="left">Langrenus (132 km wide and a max depth of 4.9 km) is just another Copernicus-style impact crater, or so it looks. Wreathed in wall terraces, and possessing a central peak complex and partly flat floor, Langrenus is Copernicus-East. Originally thought to be Copernican [[../02/LPOD-2004-02-23.htm LPOD Feb. 23]] in age (i.e. 1.1 b.y. or younger) | |
| − | + | because of its faint rays [[../04/LPOD-2004-04-16.htm LPOD Apr. 16]], crater counts show that it is late Eratosthenian, probably 1-2 b.y. old. It has also been stated as being the largest crater formed in the last 3.2 b.y., but Hausen [[../04/LPOD-2004-04-09.htm LPOD Apr. 9]] is 167 km in diameter and is also Eratosthenian. So what is left for poor Langrenus? | |
| − | + | Well, for one thing it is one of only seven craters known to have troctolite within its central peaks. Troctolite is a highlands rock type combining about equal parts olivine and plagioclase. It forms when a magnesium-rich magma remelts and assimilates highland anorthosite and cools, probably near the bottom of the lunar crust. The second unusual aspect of Langrenus is that it is the site | |
| − | + | of one of the best documented lunar transient events. The experienced French astronomer Audouin Dollfus discovered that the northern floor of Langrenus temporarily brightened when seen in polarized light on December 30, 1992 and January 2, 1993. Dollfus' interpretation was that the bright polarized areas were produced by outgassing that lifted dust above the crater floor. This is a peculiar, but well-documented observation, and is made more believable by enhanced concentrations of radon at Langrenus and nearby Fecunditatis detected during Apollo 15 and 16 missions. Perhaps the fact that the central peaks of Langrenus sampled deep crustal rocks has some connection to the proposed degassing. Have any additional polarimetric brightenings occurred since 1973? Has anyone looked? It is now within the capability of amateur imagers!<BR> | |
| − | + | </p> | |
| − | + | <blockquote> | |
| − | + | <p align="right" class="story">— [mailto:tychocrater@yahoo.com Chuck Wood]</p> | |
| − | + | </blockquote> <p><b>Technical Details:</b><br> | |
| − | + | Sept 12, 2003. 10&quot; f/6 Newtonian plus 5x barlow plus Philips Toucam Pro, 130 frames stacked. Seeing 4/10, transparency 5/10.</p> | |
| − | + | <p class="story"><b>Related Links:</b><br> | |
| − | + | [http://observingthesky.org/index.php?p=174 K.C. Pau]<br> | |
| − | + | [http://news.bbc.co.uk/1/hi/sci/tech/789095.stm Lights Glow on Moon (BBC)]</p> | |
| − | + | <p>Audouin Dollfus (2000) Lunar Surface Imaging Polarimetry. III. Langrenus, Icarus 420-429<br> | |
| − | + | Audouin Dollfus (2000) Langrenus: Transient Illuminations on the Moon, Icarus 430-443<br> | |
| − | + | Hodges, C.A. USGS I739 Geologic map of the Langrenus Quadrangle of the Moon. 1973 1:1,000,000</p> | |
| − | + | <p class="story"> <b>Tomorrow's LPOD:</b> Elger's Journal</p> | |
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| − | + | <hr> | |
| − | + | <p align="center" class="main_titles"><b>Author & Editor:</b><br> | |
| − | + | [mailto:tychocrater@yahoo.com Charles A. Wood]</p> | |
| − | + | <p align="center" class="main_titles"><b>Technical Consultant:</b><br> | |
| − | + | [mailto:anthony@perseus.gr Anthony Ayiomamitis]</p> | |
| − | + | <p align="center" class="main_titles"><b>A service of:</b><br> | |
| − | + | [http://www.observingthesky.org/ ObservingTheSky.Org]</p> | |
| − | + | <p align="center" class="main_titles"><b>Visit these other PODs:</b> <br> | |
| − | + | [http://antwrp.gsfc.nasa.gov/apod/astropix.html Astronomy] | [http://www.msss.com/ Mars] | [http://epod.usra.edu/ Earth]</p> | |
| − | + | <p> </p> | |
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===COMMENTS?=== | ===COMMENTS?=== | ||
Click on this icon [[image:PostIcon.jpg]] at the upper right to post a comment. | Click on this icon [[image:PostIcon.jpg]] at the upper right to post a comment. | ||
Revision as of 18:19, 4 January 2015
Langrenus
 |
Image Credit: K.C. Pau |
|
Langrenus Langrenus (132 km wide and a max depth of 4.9 km) is just another Copernicus-style impact crater, or so it looks. Wreathed in wall terraces, and possessing a central peak complex and partly flat floor, Langrenus is Copernicus-East. Originally thought to be Copernican [[../02/LPOD-2004-02-23.htm LPOD Feb. 23]] in age (i.e. 1.1 b.y. or younger)
because of its faint rays [[../04/LPOD-2004-04-16.htm LPOD Apr. 16]], crater counts show that it is late Eratosthenian, probably 1-2 b.y. old. It has also been stated as being the largest crater formed in the last 3.2 b.y., but Hausen [[../04/LPOD-2004-04-09.htm LPOD Apr. 9]] is 167 km in diameter and is also Eratosthenian. So what is left for poor Langrenus?
Well, for one thing it is one of only seven craters known to have troctolite within its central peaks. Troctolite is a highlands rock type combining about equal parts olivine and plagioclase. It forms when a magnesium-rich magma remelts and assimilates highland anorthosite and cools, probably near the bottom of the lunar crust. The second unusual aspect of Langrenus is that it is the site
of one of the best documented lunar transient events. The experienced French astronomer Audouin Dollfus discovered that the northern floor of Langrenus temporarily brightened when seen in polarized light on December 30, 1992 and January 2, 1993. Dollfus' interpretation was that the bright polarized areas were produced by outgassing that lifted dust above the crater floor. This is a peculiar, but well-documented observation, and is made more believable by enhanced concentrations of radon at Langrenus and nearby Fecunditatis detected during Apollo 15 and 16 missions. Perhaps the fact that the central peaks of Langrenus sampled deep crustal rocks has some connection to the proposed degassing. Have any additional polarimetric brightenings occurred since 1973? Has anyone looked? It is now within the capability of amateur imagers! Technical Details: Related Links: Audouin Dollfus (2000) Lunar Surface Imaging Polarimetry. III. Langrenus, Icarus 420-429 Tomorrow's LPOD: Elger's Journal |
Author & Editor:
Charles A. Wood
Technical Consultant:
Anthony Ayiomamitis
A service of:
ObservingTheSky.Org
Visit these other PODs:
Astronomy | Mars | Earth
COMMENTS?
Click on this icon File:PostIcon.jpg at the upper right to post a comment.
